Computer Science
Scientific paper
Jul 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.5875b&link_type=abstract
HST Proposal ID #5875
Computer Science
Hst Proposal Id #5875 Cool Stars
Scientific paper
Interest in T Tauri stars is high because they are surrounded by accretion disks like the solar nebula, and because they provide the best view of the mass loss mechanism responsible for bipolar outflows, protostellar jets, and the winds which play a big role in fixing the angular momentum and possibly the mass of the newly formed star. In Cycle 2 we obtained the first good high resolution observations of the ultraviolet emission lines formed in the interface between star and disk. These demonstrated that emission arises both in narrow components likely confined by the stellar magnetic field, and in broad components diagnostic of the accretion disk interaction with the star. There were several surprises; we did not expect material at 10^5K to so closely resemble the optical profiles. Especially tantalizing are hints that the wind itself may contain such hot material, possibly even optically thick. This has strong implications for the mechanism driving the outflow. In particular it may be difficult to produce such material in the magnetocentifugally driven winds which currently hold favor. We propose a program aimed specifically at the question of to what extent hot material exists in T Tauri winds. We will examine stars selected specifically for their wind diagnostics, and expand our coverage of stellar masses. We will also examine for the first time pre--main sequence stars without disks, to disentangle purely stellar phenomena.
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